Introduction to Tensor Calculus for General Relativity - Part I

1
Massachusetts Institute of Technology
Department o f P h ysics
Physics 8.962 Spring 2000
Introduction to Tensor Calculus for
General Relativity
c2000 Edmund Bertschinger.
1
Introduction
There are three essential ideas underlying general relativity (GR). The rst is that spacetime
may be described as a curved, four-dimensional mathematical structure called a
pseudo-Riemannian manifold. In brief, time and space together comprise a curved fourdimensional
non-Euclidean geometry. Consequently, the practitioner of GR must be
familiar with the fundamental geometrical properties of curved spacetime. In particular,
the laws of physics must be expressed in a form that is valid independently of any
coordinate system used to label points in spacetime.
The second essential idea underlying GR is that at every spacetime point there exist
locally inertial reference frames, corresponding to locally at coordinates carried by freely
falling observers, in which t h e p h ysics of GR is locally indistinguishable from that of
special relativity. This is Einstein's famous strong equivalence principle and it makes
general relativity an extension of special relativity t o a c u r v ed spacetime. The third key
idea is that mass (as well as mass and momentum ux) curves spacetime in a manner
described by the tensor eld equations of Einstein.
These three ideas are exemplied by c o n trasting GR with Newtonian gravity. I n t h e
Newtonian view, gravity is a force accelerating particles through Euclidean space, while
time is absolute. From the viewpoint of GR as a theory of curved spacetime, there is no
gravitational force. Rather, in the absence of electromagnetic and other forces, particles
follow the straightest possible paths (geodesics) through a spacetime curved by mass.
Freely falling particles dene locally inertial reference frames. Time and space are not
absolute but are combined into the four-dimensional manifold called spacetime.
In special relativity there exist global inertial frames. This is no longer true in the
presence of gravity. H o wever, there are local inertial frames in GR, such that within a

2
suitably small spacetime volume around an event (just how small is discussed e.g. in
MTW Chapter 1), one may c hoose coordinates corresponding to a nearly-at spacetime.
Thus, the local properties of special relativity c a r r y o ver to GR. The mathematics of
vectors and tensors applies in GR much as it does in SR, with the restriction that vectors
and tensors are dened independently at each spacetime event (or within a suciently
small neighborhood so that the spacetime is sensibly at).
Working with GR, particularly with the Einstein eld equations, requires some understanding
of dierential geometry. In these notes we w i l l d e v elop the essential mathematics
needed to describe physics in curved spacetime. Many p h ysicists receive their
introduction to this mathematics in the excellent boo k o f W einberg (1972). Weinbe r g
minimizes the geometrical content of the equations by representing tensors using component
notation. We believe that it is equally easy to work with a more geometrical
description, with the additional benet that geometrical notation makes it easier to distinguish
physical results that are true in any coordinate system (e.g., those expressible
using vectors) from those that are dependent on the coordinates. Because the geometry
of spacetime is so intimately related to physics, we believe that it is better to highlight
the geometry from the outset. In fact, using a geometrical approach a l l o ws us to develop
the essential dierential geometry as an extension of vector calculus. Our treatment
is closer to that Wald (1984) and closer still to Misner, Thorne and Wheeler (1973,
MTW). These books are rather advanced. For the newcomer to general relativity w e
warmly recommend Schutz (1985). Our notation and presentation is patterned largely
after Schutz. It expands on MTW Chapters 2, 3, and 8. The student wishing additional
practice problems in GR should consult Lightman et al. (1975). A slightly more
advanced mathematical treatment is provided in the excellent notes of Carroll (1997).
These notes assume familiarity with special relativity. W e will adopt units in which
the speed of light c = 1 . Greek indices (, , etc., which t a k e the range f0 1 2 3g)
will be used to represent components of tensors. The Einstein summation convention
is assumed: repeated upper and lower indices are to be summed over their ranges,
e.g., A B A 0 B 0 + A 1 B 1 + A 2 B 2 + A 3 B 3 . Four-vectors will be represented with
an arrow o ver the symbol, e.g., A, ~ while one-forms will be represented using a tilde,
e.g., B. ~ Spacetime points will be denoted in boldface type e.g., x refers to a point
with coordinates x . Our metric has signature +2 the at spacetime Minkowski metric
components are = diag(;1 +1 +1 +1).
2
Vectors and one-forms
The essential mathematics of general relativity is dierential geometry, the branch o f
mathematics dealing with smoothly curved surfaces (dierentiable manifolds). The
physicist does not need to master all of the subtleties of dierential geometry in order

3
to use general relativity. ( F or those readers who want a deeper exposure to dierential
geometry, see the introductory texts of Lovelock and Rund 1975, Bishop and Goldberg
1980, or Schutz 1980.) It is sucient to develop the needed dierential geometry as a
straightforward extension of linear algebra and vector calculus. However, it is important
to keep in mind the geometrical interpretation of physical quantities. For this reason,
we will not shy from using abstract concepts like p o i n ts, curves and vectors, and we will
distinguish between a vector A ~ and its components A . U n l i k e some other authors (e.g.,
Weinberg 1972), we will introduce geometrical objects in a coordinate-free manner, only
later introducing coordinates for the purpose of simplifying calculations. This approach
requires that we distinguish vectors from the related objects called one-forms. Once
the dierences and similarities between vectors, one-forms and tensors are clear, we will
adopt a unied notation that makes computations easy.
2.1 Vectors
We begin with vectors. A vector is a quantity with a magnitude and a direction. This
primitive concept, familiar from undergraduate physics and mathematics, applies equally
in general relativity. An example of a vector is d~x, the dierence vector between two
innitesimally close points of spacetime. Vectors form a linear algebra (i.e., a vector
~ ~
space). If A is a vector and a is a real number (scalar) then aA is a vector with the
same direction (or the opposite direction, if a < 0) whose length is multiplied by jaj. If
~ ~ ~ ~
A and B are vectors then so is A + B. These results are as valid for vectors in a curved
four-dimensional spacetime as they are for vectors in three-dimensional Euclidean space.
Note that we h a ve i n troduced vectors without mentioning coordinates or coordinate
transformations. Scalars and vectors are invariant under coordinate transformations
~
vector components are not. The whole point of writing the laws of physics (e.g., F = m~a)
using scalars and vectors is that these laws do not depend on the coordinate system
imposed by the physicist.
We denote a spacetime point using a boldface symbo l : x. (This notation is not meant
to imply coordinates.) Note that x refers to a point, not a vector. In a curved spacetime
the concept of a radius vector ~x pointing from some origin to each p o i n t x is not useful
because vectors dened at two dierent points cannot be added straightforwardly as
they can in Euclidean space. For example, consider a sphere embedded in ordinary
three-dimensional Euclidean space (i.e., a two-sphere). A v ector pointing east at one
point on the equator is seen to point radially outward at another point on the equator
whose longitude is greater by 9 0 . The radially outward direction is undened on the
sphere.
Technically, w e are discussing tangent vectors that lie in the tangent space of the
manifold at each point. For example, a sphere may b e e m bedded in a three-dimensional
Euclidean space into which m a y be placed a plane tangent to the sphere at a point. A two-

dimensional vector space exists at the point of tangency. H o wever, such a n e m bedding
is not required to dene the tangent space of a manifold (Wald 1984). As long as the
space is smooth (as assumed in the formal denition of a manifold), the dierence vector
d~x be t ween two innitesimally close points may be dened. The set of all d~x denes
the tangent space at x. By assigning a tangent v ector to every spacetime point, we
can recover the usual concept of a vector eld. However, without additional preparation
one cannot compare vectors at dierent spacetime points, because they lie in dierent
tangent spaces. In later notes we i n troduce will parallel transport as a means of making
this comparison. Until then, we consider only tangent v ectors at x. T o emphasize the
status of a tangent v ector, we will occasionally use a subscript notation: A~
X .
2.2 One-forms and dual vector space
Next we i n troduce one-forms. A one-form is dened as a linear scalar function of a vector.
That is, a one-form takes a vector as input and outputs a scalar. For the one-form P~,
P~(V~ ) is also called the scalar product and may be denoted using angle brackets:
~
P ~ (V ~ ) = hP ~ V i : (1)
The one-form is a linear function, meaning that for all scalars a and b and vectors V~ and
~W , the one-form P ~ satises the following relations:
P ~ (aV ~ + b W ~ ) = hP ~ aV ~ + b Wi ~ = ahP ~ V~ i + bhP ~ W~ i = aP ~ (V ~ ) + bP ~ ( W ~ ) : (2)
Just as we m a y consider any function f( ) as a mathematical entity independently of
any particular argument, we m a y consider the one-form P ~ independently of any particular
vector V ~ . W e m a y also associate a one-form with each spacetime point, resulting in a
one-form eld P~ = PX ~ . N o w the distinction between a point a v ector is crucial: P~ X is
a one-form at point x while P~(V~ ) is a scalar, dened implicitly at point x. The scalar
product notation with subscripts makes this more clear: hP ~ X VX ~ i.
One-forms obey their own linear algebra distinct from that of vectors. Given any t wo
scalars a and b and one-forms P~ and Q, ~ w e m a y dene the one-form aP ~ + b Q ~ by
~ Q)(V~ ) = haP~ + b ~ ~ Q ~ ~ ~ b ~ ~
(aP + b ~ Q V~ i = ahP~ V i + bh ~ V i = aP (V ) + Q(V ) : (3)
Comparing equations (2) and (3), we see that vectors and one-forms are linear operators
on each other, producing scalars. It is often helpful to consider a vector as being a linear
scalar function of a one-form. Thus, we m a y w r i t e hP ~ V~ i = P ~ (V ~ ) = V ~ (P ~ ). The set of
all one-forms is a vector space distinct from, but complementary to, the linear vector
space of vectors. The vector space of one-forms is called the dual vector (or cotangent)
space to distinguish it from the linear space of vectors (tangent space).
4

5
Although one-forms may appear to be highly abstract, the concept of dual vector
spaces is familiar to any student o f q u a n tum mechanics who has seen the Dirac bra-ket
notation. Recall that the fundamental object in quantum mechanics is the state vector,
represented by a k et j i in a linear vector space (Hilbert space). A distinct Hilbert
space is given by the set of bra vectors hj. Bra vectors and ket vectors are linear scalar
functions of each other. The scalar product hj i maps a bra vector and a ket vector to a
scalar called a probability amplitude. The distinction between bras and kets is necessary
because probability amplitudes are complex numbers. As we will see, the distinction
be t ween vectors and one-forms is necessary because spacetime is curved.
3 Tensors
Having dened vectors and one-forms we can now dene tensors. A tensor of rank (m n),
also called a (m n) tensor, is dened to be a scalar function of m one-forms and n vectors
that is linear in all of its arguments. It follows at once that scalars are tensors of rank
(0 0), vectors are tensors of rank (1 0) and one-forms are tensors of rank (0 1). We
may denote a tensor of rank (2 0) by T(P ~ Q) ~ one of rank (2 1) by T(P ~ Q ~ A), ~ etc.
Our notation will not distinguish a (2 0) tensor T from a (2 1) tensor T, although a
notational distinction could be made by placing m arrows and n tildes over the symbo l ,
or by appropriate use of dummy indices (Wald 1984).
The scalar product is a tensor of rank (1 1), which w e will denote I and call the
identity tensor:
I(P ~ V ~ ) h P ~ V ~ i = P ~ (V ~ ) = V ~ (P~) : (4)
We call ~
I the identity because, when applied to a xed one-form P ~ and any vector V , it
returns P~(V~ ). Although the identity t e n s o r w as dened as a mapping from a one-form
and a vector to a scalar, we see that it may equally be interpreted as a mapping from a
one-form to the same one-form: I(P ~ ) = P ~ , where the dot indicates that an argument
(a vector) is needed to give a scalar. A similar argument shows that I may be considered
the identity operator on the space of vectors V ~ : I( ~V ) = V~ .
A tensor of rank (m n) is linear in all its arguments. For example, for (m = 2 n = 0)
we h a ve a straightforward extension of equation (2):
T(aP ~ + b Q ~ c R ~ + dS ~ ) = ac T(P ~ R) ~ + ad T(P ~ S) ~ + bc T( Q ~ R) ~ + bd T( q ~ S ~ ) : (5)
Tensors of a given rank form a linear algebra, meaning that a linear combination of
tensors of rank (m n) is also a tensor of rank (m n), dened by straightforward extension
of equation (3). Two tensors (of the same rank) are equal if and only if they return the
same scalar when applied to all possible input vectors and one-forms. Tensors of dierent
rank cannot be added or compared, so it is important t o k eep track of the rank of each

tensor. Just as in the case of scalars, vectors and one-forms, tensor elds TX are dened
by associating a tensor with each spacetime point.
There are three ways to change the rank of a tensor. The rst, called the tensor (or
outer) product, combines two tensors of ranks (m 1 n 1) and ( m 2 n 2) to form a tensor
of rank (m 1 + m 2 n 1 + n 2 ) b y simply combining the argument lists of the two tensors
and thereby expanding the dimensionality of the tensor space. For example, the tensor
product of two v ectors A ~ and B ~ gives a rank (2 0) tensor
T = A ~ B~ T(P ~ Q) ~ A(P~) ~ B( ~ Q) ~ : (6)
We use the symbol to denote the tensor product later we will drop this symbo l f o r
notational convenience when it is clear from the context that a tensor product is implied.
Note that the tensor product is non-commutative: A ~ B ~ = 6 B ~ A ~ (unless B ~ = cA ~ for
some scalar c) because A(P~) ~ B( ~ Q) ~ = 6 A( ~ Q) ~ B(P~) ~ for all P ~ and Q. ~ W e use the symbo l
to denote the tensor product of any t wo tensors, e.g., P ~ ~ ~ ~
T = P A B is a tensor
of rank (2 1). The second way t o c hange the rank of a tensor is by c o n traction, which
reduces the rank of a (m n) tensor to (m ; 1 n ; 1). The third way is the gradient. We
will discuss contraction and gradients later.
3.1 Metric tensor
The scalar product (eq. 1) requires a vector and a one-form. Is it possible to obtain a
scalar from two v ectors or two one-forms From the denition of tensors, the answer is
clearly yes. Any tensor of rank (0 2) will give a scalar from two v ectors and any tensor
of rank (2 0) combines two one-forms to give a scalar. However, there is a particular
;1
(0 2) tensor eld gX called the metric tensor and a related (2 0) tensor eld g
X called
the inverse metric tensor for which special distinction is reserved. The metric tensor is
a symmetric bilinear scalar function of two v ectors. That is, given vectors V~ and W ~ , g
returns a scalar, called the dot product:
~ ~ ~ ~ ~
g(V ~ W ) = V W = W ~ V = g(W ~ V ) : (7)
;1
Similarly, g returns a scalar from two one-forms P ~ and Q, ~ w h ich w e also call the dot
product:
;1
g (P ~ Q) ~ = ~ ~ ~ ~ ;1
P Q = P Q = g (P ~ Q) ~ : (8)
Although a dot is used in both cases, it should be clear from the context whether g or g
;1
is implied. We reserve the dot product notation for the metric and inverse metric tensors
just as we reserve the angle brackets scalar product notation for the identity tensor (eq.
4). Later (in eq. 41) we will see what distinguishes g from other (0 2) tensors and g
;1
from other symmetric (2 0) tensors.
6

One of the most important properties of the metric is that it allows us to convert
~
vectors to one-forms. If we forget to include W in equation (7) we get a quantity, denoted
V ~ , that behaves like a one-form:
~V ( ) g(V ~ ) = g( V ~ ) (9)
where we h a ve inserted a dot to remind ourselves that a vector must be inserted to give
a scalar. (Recall that a one-form is a scalar function of a vector!) We use the same letter
to indicate the relation of V ~ and V ~ .
Thus, the metric g is a mapping from the space of vectors to the space of one-forms:
~ ~ ;1 ;1
g : V ! V . By denition, the inverse metric g is the inverse mapping: g : V ~ ! V ~ .
(The inverse always exists for nonsingular spacetimes.) Thus, if V~ is dened for any V ~
by equation (9), the inverse metric tensor is dened by
~ ~
V ( ) g
;1
(V ) = g
;1
( V ~ ) : (10)
Equations (4) and (7){(10) give us several equivalent w ays to obtain scalars from vectors
~ ~ ~
V and W and their associated one-forms V ~ and W :
hV ~ Wi ~ = hW ~ V~ i = V~ W ~ = V~ W ~ = I(V ~ W) ~ = I(W ~ V ~ ) = g(V ~ ~ ;1
W ) = g (V ~ W ~ ) : (11)
3.2 Basis vectors and one-forms
It is possible to formulate the mathematics of general relativity e n tirely using the abstract
formalism of vectors, forms and tensors. However, while the geometrical (coordinate-free)
interpretation of quantities should always be kept in mind, the abstract approach often is
not the most practical way to perform calculations. To simplify calculations it is helpful
to introduce a set of linearly independent basis vector and one-form elds spanning
our vector and dual vector spaces. In the same way, practical calculations in quantum
mechanics often start by expanding the ket vector in a set of basis kets, e.g., energy
eigenstates. By denition, the dimensionality of spacetime (four) equals the numbe r o f
linearly independent basis vectors and one-forms.
We denote our set of basis vector elds by f~e X g, where labels the basis vector
(e.g., = 0 1 2 3) and x labels the spacetime point. Any four linearly independent basis
vectors at each spacetime point will work we do not not impose orthonormality o r a n y
other conditions in general, nor have w e implied any relation to coordinates (although
later we will). Given a basis, we m a y expand any v ector eld A~
as a linear combination
of basis vectors:
~
AX = A X ~e X = A 0 X~e 0 X + A 1 X~e 1 X + A 2 X~e 2 X + A 3 X~e 3 X : (12)
7

Note our placement of subscripts and superscripts, chosen for consistency with the Einstein
summation convention, which requires pairing one subscript with one superscript.
The coecients A are called the components of the vector (often, the contravariant
~
components). Note well that the coecients A depend on the basis vectors but A does
not!
Similarly, w e m a y c hoose a basis of one-form elds in which to expand one-forms
like A~ X . Although any set of four linearly independent one-forms will suce for each
spacetime point, we prefer to choose a special one-form basis called the dual basis and
denoted fe~ X g. Note that the placement of subscripts and superscripts is signicant
we never use a subscript to label a basis one-form while we n e v er use a superscript
to label a basis vector. Therefore, e~ is not related to ~e through the metric (eq. 9):
e~ ( ) 6= g(~e ). Rather, the dual basis one-forms are dened by imposing the following
16 requirements at each spacetime point:
he~ X ~e Xi =
(13)
where
is the Kronecker delta,
= 1 if = and
= 0 otherwise, with the
same values for each spacetime point. (We m ust always distinguish subscripts from
superscripts the Kronecker delta always has one of each.) Equation (13) is a system of
four linear equations at each spacetime point for each of the four quantities e~ and it
has a unique solution. (The reader may s h o w t h a t a n y n o n trivial transformation of the
dual basis one-forms will violate eq. 13.) Now we ma y expand any one-form eld P~ X in
the basis of one-forms:
P ~ X = P X e~ X : (14)
The component P of the one-form P ~ is often called the covariant component to distin-
~
guish it from the contravariant component P
of the vector P . In fact, because we h a ve
consistently treated vectors and one-forms as distinct, we should not think of these as
being distinct "components" of the same entity a t a l l .
There is a simple way to get the components of vectors and one-forms, using the fact
that vectors are scalar functions of one-forms and vice versa. One simply evaluates the
vector using the appropriate basis one-form:
~
~
A( e~ ) = he~ Ai = he~ A ~e i = he~ ~e iA
= A
= A
(15)
and conversely for a one-form:
P ~ (~e ) = hP
~
~e i = hP e~ ~e i = he~ ~e iP = P = P : (16)
We h a ve suppressed the spacetime point x for clarity, but it is always implied.
8

3.3 Tensor algebra
We can use the same ideas to expand tensors as products of components and basis
tensors. First we note that a basis for a tensor of rank (m n) i s p r o vided by the tensor
product of m vectors and n one-forms. For example, a (0 2) tensor like the metric tensor
can be decomposed into basis tensors e~ e~ . T he components of a tensor of rank (m n),
labeled with m superscripts and n subscripts, are obtained by e v aluating the tensor using
m basis one-forms and n basis vectors. For example, the components of the (0 2) metric
tensor, the (2 0) inverse metric tensor and the (1 1) identity tensor are
;1
g g(~e ~e ) = ~e ~e g g ( e~ e~ ) = e~ e~
= I( e~ ~e ) = he~ ~e i : (17)
(The last equation follows from eqs. 4 and 13.) The tensors are given by summing over
the tensor product of basis vectors and one-forms:
;1
g = g e~
e~ g = g ~e ~e I =
~e e~
: (18)
The reader should check that equation (18) follows from equations (17) and the duality
condition equation (13).
Basis vectors and one-forms allow us to represent a n y tensor equations using components.
For example, the dot product between two v ectors or two one-forms and the
scalar product between a one-form and a vector may be written using components as
~ ~ ~ ~
A B = g A A hP~ Ai = P A P~ Q = g P P : (19)
The reader should prove these important results.
If two tensors of the same rank are equal in one basis, i.e., if all of their components
are equal, then they are equal in any basis. While this mathematical result is obvious
from the basis-free meaning of a tensor, it will have important p h ysical implications in
GR arising from the Equivalence Principle.
As we discussed above, the metric and inverse metric tensors allow us to transform
vectors into one-forms and vice versa. If we e v aluate the components of V ~ and the
one-form V~ dened by equations (9) and (10), we g e t
V = g(~e V ~ ) = g V
;1 ~
V = g ( e~ V ) = g : (20)
V
Because these two equations must hold for any v ector V~ , w e conclude that the matrix
dened by g is the inverse of the matrix dened by g :
g g = : (21)
We also see that the metric and its inverse are used to lower and raise indices on compo-
~ ~
nents. Thus, given two v ectors V and W , w e m a y e v aluate the dot product any of four
equivalent w ays (cf. eq. 11):
~ ~
V W = g V W = V W = V W = g V W : (22)
9

10
In fact, the metric and its inverse may be used to transform tensors of rank (m n)
into tensors of any rank ( m + k n ; k) where k = ;m ;m + 1 : : : n . Consider, for
example, a (1 2) tensor T with components
T T( e~ ~e ~e ) : (23)
If we fail to plug in the one-form ~e
, the result is the vector T ~e . (A one-form must be
inserted to return the quantity T .) This vector may then be inserted into the metric
tensor to give the components of a (0 3) tensor:
T g(~e T
~e ) = g T
: (24)
We could now use the inverse metric to raise the third index, say, giving us the component
of a (1 2) tensor distinct from equation (23):
T
g
;1
( e~ T e~ ) = g
T = g g T
: (25)
In fact, there are 2 m+n dierent tensor spaces with ranks summing to m + n. The metric
or inverse metric tensor allow all of these tensors to be transformed into each other.
Returning to equation (22), we see w h y we m ust distinguish vectors (with components
V ) from one-forms (with components V ). The scalar product of two v ectors requires
the metric tensor while that of two one-forms requires the inverse metric tensor. In
general, g 6= g . The only case in which the distinction is unnecessary is in at
(Lorentz) spacetime with orthonormal Cartesian basis vectors, in which ca se g =
is everywhere the diagonal matrix with entries (;1 +1 +1 +1). However, gravity curves
spacetime. (Besides, we m a y wish to use curvilinear coordinates even in at spacetime.)
As a result, it is impossible to dene a coordinate system for which g = g everywhere.
We m ust therefore distinguish vectors from one-forms and we m ust be careful about the
placement of subscripts and superscripts on components.
At this stage it is useful to introduce a classication of vectors and one-forms drawn
from special relativity with its Minkowski metric . Recall that a vector A ~ = A ~e
is called spacelike, timelike o r n ull according to whether A ~ A ~ = A A is positive,
negative or zero, respectively. In a Euclidean space, with positive denite metric, A ~ A ~
is never negative. However, in the Lorentzian spacetime geometry of special relativity,
time enters the metric with opposite sign so that it is possible to have A ~ A ~ < 0. In
particular, the four-velocity u = dx =d of a massive particle (where d is proper time)
is a timelike v ector. This is seen most simply by performing a Lorentz boost to the
z
rest frame of the particle in which c a s e u t = 1, u x = u y = u = 0 and u u = ;1.
Now, u u is a Lorentz scalar so that u ~ ~ u = ;1 i n a n y Lorentz frame. Often this is
written p~ p~ = ;m 2 where p = mu is the four-momentum for a particle of mass m.
For a massless particle (e.g., a photon) the proper time vanishes but the four-momentum

11
is still well-dened with p~ p~ = 0: the momentum vector is null. We adopt the same
notation in general relativity, replacing the Minkowski metric (components ) with the
actual metric g and evaluating the dot product using A ~ A ~ = g(A ~ A) ~ = g A A . The
;1
same classication scheme extends to one-forms using g : a one-form P ~ is spacelike,
;1
timelike o r n ull according to whether P~ P~ = g (P ~ P ~) = g P P is positive, negative
or zero, respectively. Finally, a v ector is called a unit vector if A ~ A ~ = 1 and similarly
for a one-form. The four-velocity of a massive particle is a timelike u n i t v ector.
Now that we h a ve i n troduced basis vectors and one-forms, we can dene the contraction
of a tensor. Contraction pairs two argument s o f a r a n k ( m n) tensor: one vector and
one one-form. The arguments are replaced by b a s i s v ectors and one-forms and summed
over. For example, consider the (1 3) tensor R, which m a y b e c o n tracted on its second
vector argument to give a ( 0 2) tensor also denoted R but distinguished by its shorter
argument list:
X
3
R(A ~ B) ~ = ~ B) = R( e~ A~e ~ ~
R( e~ A ~e ~ B) : (26)
In later notes we will dene the Riemann curvature tensor of rank (1 3) its contraction,
dened by equation (26), is called the Ricci tensor. Although the contracted tensor would
appear to depend on the choice of basis because its denition involves the basis vectors
and one-forms, the reader may s h o w that it is actually invariant under a change of basis
(and is therefore a tensor) as long as we use dual one-form and vector bases satisfying
equation (13). Equation (26) becomes somewhat clearer if we e x p r e s s i t e n tirely using
tensor components:
R = R : (27)
Summation over is implied. Contraction may be performed on any pair of covariant
and contravariant indices dierent tensors result.
=0